Rotating Barrow entropy-inspired wormholes versus black holes: null trajectories, shadow morphology, and exotic matter
Abstract
We construct a rotating traversable wormhole supported by a regular, entropy-inspired matter distribution and investigate its geometry, null geodesics, shadow morphology, and exotic matter content. We derive the geometry from the Barrow deformation of the Bekenstein--Hawking area law, characterized by an exponent 0<n≤1, which replaces point-like divergences with a regular matter profile. The resulting energy density is negative everywhere and scales as ρB∝−r−n−3, while the shape function smoothly satisfies the flare-out condition at the throat. We introduce slow rotation via N(r,θ)=exp[αJ2cos2θ/r2] and ω(r)=2J/r3; both remain finite at the throat, ensuring a horizon-free, traversable geometry. Equatorial null geodesics yield a photon-sphere condition distinct from the standard black-hole relation. In the static limit, the photon sphere sits at the throat, rph=rth; for slow rotation, the prograde branch moves to rph2≃ 6J, while the retrograde branch is pushed toward the throat. The critical impact parameters are ℬ±≈± rph+2J/rph. For M=1, rth=1, J/M2=0.5, this gives rph≈1.732, ℬ+≈1.90, ℬ−≈−1.55, and a fractional asymmetry 𝒜≈0.10. The weak and null energy conditions are violated, with the strongest violation near the throat, while the Barrow exponent controls the localization of exotic matter. The volume-integral quantifier IV remains finite when rthn+1=4M/[(n+2)πn/2]. Comparisons with Kerr and regular black holes indicate that shadow diameter alone may be degenerate, whereas photon-ring structure and rotational asymmetry provide complementary signatures capable of distinguishing this entropy-inspired wormhole from black-hole alternatives.
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BibTeX
@misc{errehymy2026rotating,
title = {{Rotating Barrow entropy-inspired wormholes versus black holes: null trajectories, shadow morphology, and exotic matter}},
author = {A. Errehymy and G. Yergaliyeva and S. K. Maurya and B. Turimov and I. Ibragimov and J. Rayimbaev},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.26981},
eprint = {2610.26981},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.26981},
}
RIS
TY - UNPB
TI - Rotating Barrow entropy-inspired wormholes versus black holes: null trajectories, shadow morphology, and exotic matter
AU - A. Errehymy
AU - G. Yergaliyeva
AU - S. K. Maurya
AU - B. Turimov
AU - I. Ibragimov
AU - J. Rayimbaev
PY - 2026
DA - 2026/10/19
PB - arXiv
DO - 10.48550/arxiv.2610.26981
UR - https://arxiv.org/abs/2610.26981
AB - We construct a rotating traversable wormhole supported by a regular, entropy-inspired matter distribution and investigate its geometry, null geodesics, shadow morphology, and exotic matter content. We derive the geometry from the Barrow deformation of the Bekenstein--Hawking area law, characterized by an exponent 0<n≤1, which replaces point-like divergences with a regular matter profile. The resulting energy density is negative everywhere and scales as ρ_B∝−r^−n−3, while the shape function smoothly satisfies the flare-out condition at the throat. We introduce slow rotation via N(r,θ)=exp[αJ^2cos^2θ/r^2] and ω(r)=2J/r^3; both remain finite at the throat, ensuring a horizon-free, traversable geometry. Equatorial null geodesics yield a photon-sphere condition distinct from the standard black-hole relation. In the static limit, the photon sphere sits at the throat, r_ph=r_th; for slow rotation, the prograde branch moves to r_ph^2≃ 6J, while the retrograde branch is pushed toward the throat. The critical impact parameters are ℬ_±≈± r_ph+2J/r_ph. For M=1, r_th=1, J/M^2=0.5, this gives r_ph≈1.732, ℬ_+≈1.90, ℬ_−≈−1.55, and a fractional asymmetry 𝒜≈0.10. The weak and null energy conditions are violated, with the strongest violation near the throat, while the Barrow exponent controls the localization of exotic matter. The volume-integral quantifier I_V remains finite when r_th^n+1=4M/[(n+2)π^n/2]. Comparisons with Kerr and regular black holes indicate that shadow diameter alone may be degenerate, whereas photon-ring structure and rotational asymmetry provide complementary signatures capable of distinguishing this entropy-inspired wormhole from black-hole alternatives.
ER -